Lecture 8: Stellar Motions
Reading: Box 19-1
Key Ideas
The stars are in constant
motion.
Observed Motions
Proper motions (motion
against the background, measured in angular motion/time)
Radial velocities (motion
towards or away, measured from the Doppler shift)
True Space Motion
Combination of radial
velocity, proper motion, and distance (important for proper motion!)
The ÒFixedÓ Stars
Although the stars are
moving, their motions across the sky are so small that to the naked eye, the
stars appear ÒfixedÓ to the sky.
Great distances make the amount of motion small on human lifetimes. (Of
course, stars moving directly away or towards us will not to appear to move
across the sky)
Proper Motions
Apparent angular motion
across the sky of nearby stars with respect to distant objects. (Distant stars
are used because we assume that even though they are moving through space they
are so far away that from our perspective they are fixed). It is the projection
of the starÕs true motion through space relative to the Sun.
Typical proper motion for
stars in the solar neighborhood is about 0.1 arcsec/year
Largest proper motion
measured is 10.25 arcsec/year BarnardÕs Star)
Proper motions are
cumulative.
Effects build up over time.
The longer you wait, the greater apparent angular motion is.
Measuring proper motions:
Compare photos of the sky
taken 20 to 50 years apart
Measure how much stars have
moved compared to more distant background objects (galaxies, quasars).
Example: if a star has a
proper motion of 0.1 arcsec/year:
In one year, it moves 0.1
arcsec
In 10 years, it moves 10x0.1=
1 arcsec
In 100 years, it moves
100x0.1 =10 arcsec
It can take a long time for
the constellations to noticeably change shape.
History: Edmund Halley
Example: the Big Dipper
Proper Motion depends on
Distance
For the same actual distance
traveled by a star, a star that is closer to the Sun will appear to move a larger angular distance.
More distant stars tend to
have smaller proper motions.
Can usually measure accurate
proper motions out to distances of about 1000 parsecs.
Distance is not the only
reason why stars with large velocities can appear to have very small proper
motions.
Stars moving exactly along
the line of sight have no proper motion.
Radial Velocity
However, we can measure the
speed along the line of sight using the Doppler shift.
Note that the velocity
measured from the Doppler shift does NOT depend on distance. Indeed we can
measure radial velocity out to the edge of the visible Universe if we get enough
photons.
True Space Motion
Now that weÕve measured the
radial velocity and the tangential velocity (proper motion x distance), we can
figure out the true space motion of the object.
The gory details of true
space motion:
Radial velocity (vr):
from Doppler Shift
Tangential velocity (vt):
from Proper Motion and Distance:
vt=4.74md
m is the proper motion in arcsec/year
d is distance in parsecs
vt is the
tangential velocity in km/sec
Finally we can get the true
space velocity from the Pythagorean Theorem
Why measure space motions?
Most useful when measured for
many stars.
Use the statistics of the
motions to find:
Motion of Sun
through nearby space (towards the constellation Hercules)
Location rotation of
the Milky Way galaxy
Identify
odd-ball stars that move ÒpeculiarlyÓ relative to otherwise similar stars.
Kicked
by explosion?
Visitors
from outer reaches of Milky Way?
Important tool for studying
the structure of the Milky Way galaxy.